The growth of matter perturbations in

RADOUANE GANNOUJI , B. Moraes, D. Polarski

Research output: Contribution to journalArticlepeer-review

96 Scopus citations


We consider the linear growth of matter perturbations on low redshifts in some f(R) dark energy (DE) models. We discuss the definition of dark energy (DE) in these models and show the differences with scalar-tensor DE models. For the f(R) model recently proposed by Starobinsky we show that the growth parameter γ 0≡γ(z = 0) takes the value γ 0 0.4 for Ω m,0 = 0.32 and γ 0 0.43 for Ω m,0 = 0.23, allowing for a clear distinction from ΛCDM. Though a scale-dependence appears in the growth of perturbations on higher redshifts, we find no dispersion for γ(z) on low redshifts up to z ∼ 0.3, γ(z) is also quasi-linear in this interval. At redshift z = 0.5, the dispersion is still small with Δγ 0.01. As for some scalar-tensor models, we find here too a large value for γ′ 0≡(dγ/dz)(z = 0), γ′ 0 -0.25 for Ω m,0 = 0.32 and γ′ 0 -0.18 for Ω m,0 = 0.23. These values are largely outside the range found for DE models in General Relativity (GR). This clear signature provides a powerful constraint on these models. 2009 IOP Publishing Ltd and SISSA.

Original languageEnglish
Article number034
JournalJournal of Cosmology and Astroparticle Physics
Issue number2
StatePublished - 25 May 2009


  • Cosmological perturbation theory
  • Dark energy theory

Fingerprint Dive into the research topics of 'The growth of matter perturbations in'. Together they form a unique fingerprint.

Cite this